• 천문학회보
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• 제36권1호
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• pp.58.1-58.1
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• 2011

We present elemental abundances of 95 blue compact dwarf galaxies (BCDs) at z=0.2~0.35 using the Sloan Digital Sky Survey (SDSS) DR7. We derived element abundances using Te method. We found that nitrogen abundance of merging BCDs are more enriched than normal BCDs by fast rotating young massive star. On the other hand, neon and oxygen abundances for merging BCDs are slightly lower than the normal BCDs. This might be result from the dilution by metal-poor gas infall during the interaction. This means that merging BCDs undergone star formation event for a long time than normal BCDs and we trying to explain using STARLIGHT code and various star formation rates (SFRs) ratios. At a result, merging BCDs have older stellar population (>10 Myr) more than normal BCDs and have clear distinction in elements abundances versus Ha/UV diagram. We also discuss the characteristics of post merger candidate using FUV to NUV ratios.

• 대한전기학회:학술대회논문집
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• 대한전기학회 1987년도 전기.전자공학 학술대회 논문집(I)
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• pp.429-432
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• 1987

A new LOCOS (Local Oxidation of Silicon) process using a thin nitride film directly deposited on the silicon substrate by LPCVD has been developed in order to reduce the bird's beak length. SEM studies showed that nitride thickness of 50nm can decrease the bird's beak length down to 0.2um with 450nm field oxide. No crystalline defects are observed around the bird's beak after the Wright etch. A 30% improvement in current density was obtained when this new method was applied to MOS transistors (W/L*2.9/20.4) compared to conventional LOCOS process (bird's beak length=0.7um). Other various electrical parameters improved by this new simple LOCOS process are reported in this paper.

• 한국정보과학회:학술대회논문집
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• 한국정보과학회 2002년도 가을 학술발표논문집 Vol.29 No.2 (1)
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• pp.190-192
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• 2002

데이터 웨어하우스는 기업의 의사 결정을 지원하기 위해 기업의 운영 데이터베이스로부터 추출한 데이터의 집합으로써 OLAP 분석에 이용된다. OLAP은 데이터에 대한 다양한 분석을 위해 이들 데이터를 다차원 데이터 모델로 표현하고 이를 활용하여 복잡한 질의 처리 및 다차원 데이터 분석에 이용한다. 이러한 OLAP의 다차원 데이터를 관계형 데이터베이스에서 표현하기 위해 스타 스키마가 널리 사용된다. 지금까지의 데이터 웨어하우스는 일반적으로 ER 도형으로 설계된 소스 데이터로부터 스타 스키마를 설계하고 구축하였다. 하지만, 최근 인터넷의 급성장으로 인해 차세대 웹 문서의 표준인 XML을 통한 인터넷 상의 문서 전송 및 정보 교환이 활발해 지고 있으며, XML 문서에 대한 다차원적인 분석이 요구됨에 따라 데이터 웨어하우스는 XML 문서로부터의 스타 스키마 설계 및 저장이 필요하게 되었다. 따라서 본 논문에서는 XML DTD로부터 애트리뷰트 트리를 생성하여 스타 스키마를 설계하고 이 DTD를 따르는 XML 문서에서 스타 스키마의 인스턴스를 추출하여 관계형 데이터베이스에 저장하기 위한 XML2Star 알고리즘을 개발하였다. 이것을 통해 기업 및 사용자는 OLAP에서 XML 기반의 스타 스키마를 이용한 다차원적인 분석이 가능하게 된다.

• 충청수학회지
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• 제24권4호
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• pp.807-824
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• 2011

It has been proved that if $\mathbb{X}^{(s,s)}$ is the union of two linear star-configurations in $\mathbb{P}^2$ of type $s{\times}s$, then $(I_{\mathbb{X}^{(s,s)}})_s{\neq}\{0\}$ for s = 3, 4, 5, and $(I_{\mathbb{X}^{(s,s)}})_s=\{0\}$ for $s{\geq}6$. We extend $\mathbb{P}^2$ to $\mathbb{P}^n$ and show that if $\mathbb{X}^{(s,s)}$ is the union of two linear star-configurations in $\mathbb{P}^n$, then $(I_{\mathbb{X}^{(s,s)}})_s=\{0\}$ for $n{\geq}3$ and $s{\geq}3$. Using this generalization, we also prove that the secant variety $Sec_1(Split_s(\mathbb{P}^n))$ has the expected dimension 2ns + 1 for $n{\geq}3$ and $s{\geq}3$.

• 천문학회지
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• 제52권3호
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• pp.83-88
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• 2019

Using ALMA observations of the $^{13}CN$ and DCN lines in the massive star-forming region G33.92+0.11A, we investigate the CN/HCN abundance ratio, which serves as a tracer of photodissociation chemistry, over the whole observed region. Even considering the uncertainties in calculating the abundance ratio, we find high ratios (${\gg}1$) in large parts of the source, especially in the outer regions of star-forming clumps A1, A2, and A5. Regions with high CN/HCN ratios coincide with the inflows of accreted gas suggested by Liu et al. (2015). We conclude that we found strong evidence for interaction between the dense gas clumps and the accreted ambient gas which may have sequentially triggered the star formation in these clumps.

• 천문학회보
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• 제44권1호
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• pp.77.2-77.2
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• 2019

NGC 4522 is one of the best-known examples among the Virgo galaxies undergoing active ram pressure stripping. There have been a number of detailed observational and theoretical studies on this galaxy to constrain its stripping and star formation history. However, the impact of ram pressure on the multi-phased ISM, in particular molecular gas which plays an important role in star formation, is still not fully understood. NGC 4522, as a system where the extra-planar molecular gas is identified, is an ideal case to probe in depth how ram pressure affects molecular gas properties. Aiming to get more theoretical insights on the detailed stripping process of multi-phased ISM and its consequences, we have conducted simulations using the TIGRESS which could reproduce the realistic ISM under comparable conditions as NGC 4522. In this work, we compare the fraction of gas mass to stellar mass, star formation rates and gas depletion time scales of NGC 4522 with those measured from the simulations, not only inside the disk but also in the extra-planar space.

• 천문학회보
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• 제43권2호
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• pp.40.1-40.1
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• 2018

Among Type I supernovae, which show no evidence for hydrogen lines in spectra, Type Ib/c supernovae lack of strong Si absorption lines and are involved with massive progenitors. While strong helium absorption lines are present in Type Ib supernovae, narrow helium emission lines also can appear in some Type Ib that are often called Type Ibn supernovae (SNe Ibn). We consider helium giant stars as a promising progenitor candidate for SN Ibn and suggest the evolutionary scenario through binary systems using MESA code. In our models the range of primary mass is 11 - 20 solar mass, mass ratio is 0.5 - 0.9, and initial period is 1.5 / 1.7 / 2.0 / 2.5 / 3.0 day. In particular, we find that the evolution of the secondary star can overtake the primary through mass transfer from the secondary to the primary, which is so-called 'reverse case B' mass transfer. In such systems the secondary star may undergo a supernova explosion earlier than the primary star. In this case, the primary star evolves towards a single helium giant to become a SN Ibn progenitor. These cases are more frequent in relatively low initial primary mass.

• 월간포장계
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• 통권361호
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• pp.48-63
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• 2023

산업통상자원부가 주최하고 한국생산기술연구원 패키징기술센터가 주관하는 '제 17회 대한민국 패키징 대전(KOREA STAR AWARDS 2023)'은 국내 패키징(포장) 산업의 기술개발 및 패키징 산업 발전에 기여한 유공자를 발굴하여 포상함으로써 관련 종사자의 사기 진작 및 기술 개발 의욕을 고취하고, 국내 제조업의 경쟁력을 높이기 위해 기획되었다. 올해 포상은 기업부문(34곳), 학생부문(43팀), 공로부문(2명)으로 나뉘어 총 79명(팀)이 수상의 영광을 안았다. 수상자들에게는 ASIA STAR AWARDS 2023, WORLD STAR AWARDS 2024 등 해외 패키징 포상제도 출품 자격이 부여되며, 수상홍보 및 각종 전시회 참가 지원이 이뤄진다. 지면에서는 2023년 수상작 중 기업부문 상품을 자세히 살펴보도록 한다. 이번 수상작들이 신제품으로 출품되고, 창업 아이템으로 활용되며 나아가 패키징의 변화를 이끄는 데 긍정적인 영향으로 이어지길 희망한다. 다시 한번 2023 대한민국 패키징 대전의 영예로운 수상을 축하드린다.

• 천문학회보
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• 제45권1호
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• pp.42.1-42.1
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• 2020

Filamentary structures pervade the whole kind of molecular clouds from low- to high-mass star-forming clouds, and the non-star-forming clouds. It is supposed to be a prerequisite stage of star formation, and hence how filaments and dense cores form is one of the critical questions in the early star formation study. We investigated the dynamics and chemistry of dense cores in IC5146 using TRAO FUNS (TRAO Survey of the nearby Filamentary molecular clouds, the Universal Nursery of Stars) data. In addition, we performed polarization observation using JCMT Pol-2 polarimetry to investigate the magnetic field morphology within a core-scale. In the presentation, we will present the result of TRAO FUNS and JCMT/Pol2 observation toward the filaments and dense cores in the IC5146. We aim to reveal the roles of gravity, turbulence, and magnetic field in the formation of dense cores in the western hub-filament structure of IC5146.

• 천문학회보
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• 제46권1호
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• pp.54.1-54.1
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• 2021

Observing sub-mm continuum emission from cold dust can play an important role in measuring star formation rates of galaxies, especially in the case of AGN host ones, since AGNs contaminate FIR fluxes by dust heating. To measure star formation rates, we observed total 49 local AGN host galaxies(z<0.2) by SCUBA-2 camera at James Clerk Maxwell Telescope(JCMT) at 450㎛ and 850㎛. We performed several tests with the observed images to determine whether each source is detected, and adopted 3s as the flux upper limit in non-detection cases. Using these measurements and FIR archival data, we modeled spectral energy distributions of the galaxies to estimate star formation rates. The effect of AGN activity on host galaxy star formation will be discussed.